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26. Dark Matter 1 26 26. Dark matter 1 26. DARK MATTER Revised September 2015 by M. Drees (Bonn University) and G. Gerbier (Queen’s University, Canada). 26.1. Theory 26.1.1. Evidence for Dark Matter : The existence of Dark (i.e., non-luminous and non-absorbing) Matter (DM) is by now well established [1,2]. The earliest, and perhaps still most convincing, evidence for DM came from the observation that various luminous objects (stars, gas clouds, globular clusters, or entire galaxies) move faster than one would expect if they only felt the gravitational attraction of other visible objects. An important example is the measurement of galactic rotation curves. The rotational velocity v of an object on a stable Keplerian orbit with radius r around a galaxy scales like v(r) M(r)/r, where p M(r) is the mass inside the orbit. If r lies outside the visible part of the∝ galaxy and mass tracks light, one would expect v(r) 1/√r. Instead, in most galaxies one finds that v becomes approximately constant out∝ to the largest values of r where the rotation curve can be measured; in our own galaxy, v 240 km/s at the location of our solar system, with little change out to the largest observable≃ radius. This implies the existence of a dark halo, with mass density ρ(r) 1/r2, i.e., M(r) r; at some point ρ will have to fall off faster (in order to keep the∝ total mass of the galaxy∝ finite), but we do not know at what radius this will happen. This leads to a lower bound on the DM mass density, ΩDM > 0.1, where ΩX ρX /ρcrit, ρcrit being the critical mass density (i.e.,Ωtot = 1 corresponds∼ to a flat Universe).≡ The observation of clusters of galaxies tends to give somewhat larger values, ΩDM 0.2. These observations include measurements of the peculiar velocities of galaxies in≃ the cluster, which are a measure of their potential energy if the cluster is virialized; measurements of the X-ray temperature of hot gas in the cluster, which again correlates with the gravitational potential felt by the gas; and—most directly—studies of (weak) gravitational lensing of background galaxies on the cluster. A particularly compelling example involves the bullet cluster (1E0657-558) which recently (on cosmological time scales) passed through another cluster. As a result, the hot gas forming most of the clusters’ baryonic mass was shocked and decelerated, whereas the galaxies in the clusters proceeded on ballistic trajectories. Gravitational lensing shows that most of the total mass also moved ballistically, indicating that DM self-interactions are indeed weak [1]. Many cosmologists consider the existence of old galaxies (detected at redshift z 10) to be the strongest argument for the existence of DM. Observations of the cosmic∼ microwave background (CMB) show that density perturbations at z 1, 300 were very small, δρ/ρ < 10−4. Since (sub–horizon sized) density perturbations≃ grow only in the matter–dominated epoch, and matter domination starts earlier in the presence of DM, density perturbations start to grow earlier when DM is present, therefore allowing an earlier formation of the first galaxies [3]. C. Patrignani et al. (Particle Data Group), Chin. Phys. C, 40, 100001 (2016) October 1, 2016 19:59 2 26. Dark matter All these arguments rely on Einsteinian, or Newtonian, gravity. One might thus ask whether the necessity to postulate the existence of DM, sometimes perceived to be ad hoc, could be avoided by modifying the theory of gravity. Indeed, the so–called Modified Newtonian Dynamics (MOND) allows to reproduce many observations on galactic scales, in particular galactic rotation curves, without introducing DM [4]. However, MOND is a purely non–relativistic theory. Attempts to embed it into a relativistic field theory require the existence of additional fields (e.g. a vector field or a second metric), and introduce considerably arbitrariness [4]. Moreover, the correct description of large–scale structure formation seems to require some sort of DM even in these theories [5]. In contrast, successful models of particle DM (see below) can be described in the well established language of quantum field theory, and do not need any modification of General Relativity, which has passed a large number of tests with flying colors [6]. The currently most accurate, if somewhat indirect, determination of ΩDM comes from global fits of cosmological parameters to a variety of observations; see the Section on Cosmological Parameters for details. For example, using measurements of the anisotropy of the cosmic microwave background (CMB) and of the spatial distribution of galaxies, Ref. 7 finds a density of cold, non-baryonic matter 2 Ωnbmh =0.1186 0.0020 , (26.1) ± where h is the Hubble constant in units of 100 km/(s Mpc). Some part of the baryonic matter density [7], · 2 Ωbh =0.02226 0.00023 , (26.2) ± may well contribute to (baryonic) DM, e.g., MACHOs [8] or cold molecular gas clouds [9]. The DM density in the “neighborhood” of our solar system is also of considerable interest. This was first estimated as early as 1922 by J.H. Jeans, who analyzed the motion of nearby stars transverse to the galactic plane [2]. He concluded that in our galactic neighborhood, the average density of DM must be roughly equal to that of luminous matter (stars, gas, dust). Remarkably enough, a recent estimate finds a quite similar result for the smooth component of the local Dark Matter density [10]: local GeV ρ = (0.39 0.03) (1.2 0.2) (1 δtriax) . (26.3) DM ± · ± · ± cm3 The first term on the right-hand side of Eq. (26.3) gives the average Dark Matter density at a point one solar distance from the center of our galaxy. The second factor accounts for the fact that the baryons in the galactic disk, in which the solar system is located, also increase the local DM density [11]. The third factor in Eq. (26.3) corrects for possible deviations from a purely spherical halo; according to [12], δtriax 0.2. Small substructures (minihaloes, streams) are not likely to change the local DM≤ density significantly [1]. Note that the first factor in Eq. (26.3) has been derived by fitting a complete model of our galaxy to a host of data, including the galactic rotation curve. A “purely local” analysis, only using the motion of nearby stars, gives a consistent result, with an error three times as large [13]. October 1, 2016 19:59 26. Dark matter 3 26.1.2. Candidates for Dark Matter : Analyses of structure formation in the Universe indicate that most DM should be “cold” or “cool”, i.e., should have been non-relativistic at the onset of galaxy formation (when there was a galactic mass inside the causal horizon) [1]. This agrees well with the upper bound [7] on the contribution of light neutrinos to Eq. (26.1), 2 Ωνh 0.0062 95% CL . (26.4) ≤ Candidates for non-baryonic DM in Eq. (26.1) must satisfy several conditions: they must be stable on cosmological time scales (otherwise they would have decayed by now), they must interact very weakly with electromagnetic radiation (otherwise they wouldn’t qualify as dark matter), and they must have the right relic density. Candidates include primordial black holes, axions, sterile neutrinos, and weakly interacting massive particles (WIMPs). Primordial black holes must have formed before the era of Big-Bang nucleosynthesis, since otherwise they would have been counted in Eq. (26.2) rather than Eq. (26.1). Such an early creation of a large number of black holes is possible only in certain somewhat contrived cosmological models [14]. The existence of axions [15] was first postulated to solve the strong CP problem of QCD; they also occur naturally in superstring theories. They are pseudo Nambu- Goldstone bosons associated with the (mostly) spontaneous breaking of a new global “Peccei-Quinn” (PQ) U(1) symmetry at scale fa; see the Section on Axions in this Review for further details. Although very light, axions would constitute cold DM, since they were produced non-thermally. At temperatures well above the QCD phase transition, the axion is massless, and the axion field can take any value, parameterized by the “misalignment angle” θi. At T < 1 GeV, the axion develops a mass ma fπmπ/fa due to instanton effects. Unless the∼ axion field happens to find itself at the∼ minimum of its potential (θi = 0), it will begin to oscillate once ma becomes comparable to the Hubble parameter H. These coherent oscillations transform the energy originally stored in the axion field into physical axion quanta. The contribution of this mechanism to the present axion relic density is [1] 1 175 2 12 . 2 Ωah = κa ³fa/10 GeV´ θi , (26.5) where the numerical factor κa lies roughly between 0.5 and a few. If θi (1), 11 ∼ O Eq. (26.5) will saturate Eq. (26.1) for fa 10 GeV, comfortably above laboratory and astrophysical constraints [15]; this would∼ correspond to an axion mass around 0.1 meV. However, if the post-inflationary reheat temperature TR > fa, cosmic strings will form during the PQ phase transition at T fa. Their decay will give an additional ≃ contribution to Ωa, which is often bigger than that in Eq. (26.5) [1], leading to a smaller preferred value of fa, i.e., larger ma. On the other hand, values of fa near the Planck scale become possible if θi is for some reason very small. “Sterile” SU(2) U(1)Y singlet neutrinos with keV masses [16] could alleviate the “cusp/core problem”× [1] of cold DM models.
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